The plasma cools as it rises and descends in the narrow spaces between the granules.

The plasma will cool.

When the plasma rapidly cools falling down towards the photosphere, we have the chromospheric condensation.

The plasma may cool rapidly in this region (for a thermal instability), creating dark filaments in the solar disk or prominences off the limb.

The sky darkened suddenly, as if the hidden sun had been eclipsed; the plasma must have cooled enough to start forming nitric oxides.

Eddington, however, wondered what would happen when this plasma cooled and the energy which kept the atoms ionized was no longer present.

The glare was a sparkling echo to the southern aurora where plasma from the bunker's destruction cooled and dissipated in a broad cloud.

This plasma cooled as the universe expanded, and when it cooled enough to form stable atoms it no longer absorbed the photons.

As the plasma cools, the atoms react, forming fine droplets and then solid particles of oxides.

In order to maintain the fusion process, particles from the hot plasma must be confined in the central region, or the plasma will rapidly cool.